Analysis of the spiral structure in a simulated galaxy

Abstract

We analyze the spiral structure that results in a numerical simulation of a galactic disk with stellar and gaseous components evolving in a potential that includes an axisymmetric halo and bulge. We perform a second simulation without the gas component to observe how it affects the spiral structure in the disk. To quantify this, we use a Fourier analysis and obtain values for the pitch angle and the velocity of the self-excited spiral pattern of the disk. The results show a tighter spiral in the simulation with gaseous component. The spiral structure is consistent with a superposition of waves, each with a constant pattern velocity in given radial ranges.

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Cited by in corpus (5)

• Spiral arm formation mechanisms: Spiral Structure in Barred galaxies. Observational constraints to spiral arm formation mechanisms
• Testing Hydrodynamics Schemes in Galaxy Disc Simulations
• Global Spiral Arms Formation by Non-linear Interaction of Wakelets
• Revealing the spiral arms through radial migration and the shape of the Metallicity Distribution Function
• Classifying and modelling spiral structures in hydrodynamic simulations of astrophysical discs